Notes:
- 1) The fitting includes the systematic errors.
- 2) When the burst includes telescope slew time periods, the fitting uses an average response file made from multiple 5-s response files through out the slew time plus single time preiod for the non-slew times, and weighted by the total counts in the corresponding time period using addrmf. An average response file is needed becuase a spectral fit using the pre-slew DRM will introduce some errors in both a spectral shape and a normalization if the PHA file contains a lot of the slew/post-slew time interval.
- 3) For fits to more complicated models (e.g. a power-law over a cutoff power-law), the BAT team has decided to require a chi-square improvement of more than 6 for each extra dof.
Time averaged spectrum fit using the average DRM
Power-law model
Time interval is from -7.044 sec. to 10.868 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.03639 ( -0.128216 0.124096 )
Norm@50keV : 6.16328E-03 ( -0.000483306 0.000475738 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.36 using 59 PHA bins.
# Reduced chi-squared = 1.024 for 57 degrees of freedom
# Null hypothesis probability = 4.250441e-01
Photon flux (15-150 keV) in 17.91 sec: 0.940380 ( -0.060763 0.06085 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.02039e-06 ( -7.40736e-08 7.48928e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -7.044 sec. to 10.868 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.82652 ( -0.281602 0.508529 )
Epeak [keV] : 36.5453 ( )
Norm@50keV : 8.04746E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.77 using 59 PHA bins.
# Reduced chi-squared = 1.032 for 56 degrees of freedom
# Null hypothesis probability = 4.095863e-01
Photon flux (15-150 keV) in 17.91 sec: 0.929891 ( -0.064852 0.064653 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.196 sec. to 0.804 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.72493 ( -0.146312 0.142265 )
Norm@50keV : 2.51720E-02 ( -0.00230686 0.00228199 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 68.73 using 59 PHA bins.
# Reduced chi-squared = 1.206 for 57 degrees of freedom
# Null hypothesis probability = 1.372523e-01
Photon flux (15-150 keV) in 1 sec: 3.37293 ( -0.28658 0.28681 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.3267e-07 ( -2.20644e-08 2.22771e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.196 sec. to 0.804 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.05344 ( -0.572383 0.653394 )
Epeak [keV] : 68.4196 ( -15.0139 98.8099 )
Norm@50keV : 5.62287E-02 ( -0.0273744 0.064065 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.63 using 59 PHA bins.
# Reduced chi-squared = 1.154 for 56 degrees of freedom
# Null hypothesis probability = 2.007335e-01
Photon flux (15-150 keV) in 1 sec: 3.28812 ( -0.2967 0.29591 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.23254e-07 ( -2.33599e-08 2.36568e-08 ) ergs/cm2
Time-resolved spectra
